Download The Sagittarius dwarf irregular galaxy: Metallicity and stellar

Astronomy
&
Astrophysics
A&A 384, 393–402 (2002)
DOI: 10.1051/0004-6361:20020047
c ESO 2002
The Sagittarius dwarf irregular galaxy: Metallicity and stellar
populations?
Y. Momany1,2 , E. V. Held3 , I. Saviane4 , and L. Rizzi3,2
1
2
3
4
European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
Dipartimento di Astronomia, Università di Padova, vicolo dell’Osservatorio 2, 35122 Padova, Italy
Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy
e-mail: held, [email protected]
European Southern Observatory, Casilla 19001, Santiago 19, Chile
e-mail: [email protected]
Received 1 August 2001 / Accepted 2 January 2002
Abstract. We present deep BV I observations of the dwarf irregular galaxy UKS 1927-177 in Sagittarius (SagDIG).
Statistically cleaned V , (B − I) color-magnitude diagrams clearly display the key evolutionary features in this
galaxy. Previously detected C stars are located in the color-magnitude diagrams and shown to be variable, thus
confirming the presence of a significant upper-AGB intermediate age population. A group of likely red supergiants
is also identified, whose magnitude and color is consistent with a 30 Myr old burst of star formation. The observed
colors of both blue and red stars in SagDIG are best explained by introducing a differential reddening scenario
in which internal dust extinction affects the star forming regions. Adopting a low reddening for the red giants,
E(B −V ) = 0.07±0.02, gives [Fe/H] = −2.1±0.2 for the mean stellar metallicity, a value consistent with the [O/H]
abundance measured in the Hii regions. This revised metallicity, which is in accord with the trend of metallicity
against luminosity for dwarf irregular galaxies, is indicative of a “normal”, although metal-poor, dIrr galaxy. A
quantitative description is given of the spatial distribution of stars in different age intervals, in comparison with
the distribution of the neutral hydrogen. We find that the youngest stars are located near the major peaks of
emission on the Hi shell, whereas the red giants and intermediate-age C stars define an extended halo or disk with
scale length comparable to the size of the hydrogen cloud. The relationship between the distribution of ISM and
star formation is briefly discussed.
Key words. galaxies: fundamental parameters – galaxies: individual: UKS 1927-177 – galaxies: dwarf –
galaxies: local group – Galaxy: stellar content
1. Introduction
The Sagittarius dwarf irregular (dIrr) galaxy, also known
as SagDIG or UKS 1927-177, is a quite difficult object
to study because of its low Galactic latitude and consequent high foreground contamination. First reported
by Cesarsky et al. (1977) on ESO Schmidt photographic
plates, the galaxy was studied by Longmore et al.
(1978), who derived a total luminosity MB = −10.5.
The first CCD study of the resolved star content in
SagDIG was that of Cook (1987; hereafter C87), who obtained both intermediate-band and broad-band photometry. Recently, two new investigations have improved our
knowledge of the distance and stellar content of this galaxy
(Karachentsev et al. 1999; Lee & Kim 2000; hereafter
Send offprint requests to: Y. Momany,
e-mail: [email protected]
?
Based on data collected at the European Southern
Observatory, La Silla, Chile, prop. No. 63.N-0024.
KAM99 and LK00 respectively). A new distance modulus was derived from the tip of the RGB, equal to
(m − M )0 = 25.13 in KAM99 and (m − M )0 = 25.36 in
LK00, respectively. This distance indicates that SagDIG
is a member of the Local Group (LG), confirming the evidence from its negative radial velocity and position in
the V vs. cos θ diagram (van den Bergh 1994; Pritchet &
van den Bergh 1999). Both studies, while adopting different estimates for the reddening, concluded that SagDIG
has the lowest metallicity among the LG star forming
dwarf galaxies (KAM99 estimated [Fe/H] ∼ −2.45, while
LK00 give [Fe/H] in the range −2.8 to −2.4; both estimates are based on an extrapolation of the calibration
relation for Galactic globular clusters).
The cold and warm interstellar medium (ISM) of
SagDIG and its kinematics have been the subject of several investigations. Skillman et al. (1989b) obtained optical spectrophotometry of the most luminous Hii regions,
and estimated a [O/H] abundance ∼3% of the solar value.
Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20020047
394
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
New measurements of the O and N abundance in the Hii
regions of SagDIG are presented in a companion paper
(Saviane et al. 2001). The new estimate, 12 + log(O/H) =
7.23 ± 0.20, is by 0.2 dex more metal-poor than found by
Skillman et al. (1989b). The photometric properties of the
Hii regions were investigated by Strobel et al. (1991), who
detected 3 regions in their 2.0 5 square field.
High-resolution, high sensitivity VLA observations of
the SagDIG Hi content have been obtained by Young &
Lo (1997) (see also Lo et al. 1993). About 1.2 × 107 M of
H+He have been estimated (using the new distance from
KAM99 and the Hi mass from Young & Lo), distributed
in an almost symmetric ring likely produced by the combined effects of stellar winds and supernovae. SagDIG thus
appears to have a high mass fraction in the form of neutral gas, MHI /LB = 1.6, a value quite typical of the Hi
content in dwarf irregular galaxies (see Mateo 1998).
Because of its high gas content, low luminosity, and
especially its claimed very low metallicity, SagDIG may
be a clue to the origin and evolution of dwarf galaxies.
Although located at the border of the Local Group it is
still close enough to allow us to study both its stellar populations and the gaseous component, and to compare their
physical properties. In particular, a sound knowledge of
the metallicity of SagDIG is important to constrain the
luminosity-metallicity relation for dIrrs at the metal-poor
end, and to trace the metal enrichment history in dwarf
galaxies. All this motivated an independent study of the
metallicity, distance, and stellar content of SagDIG. The
large baseline provided by the (B − I) color, together with
an analysis based on statistical subtraction of the Galactic
foreground, allowed us to improve the discrimination of
young and old stellar populations in the color-magnitude
diagram (CMD). By accounting for the differential effects
of internal dust extinction, we revise upward the [Fe/H]
estimate and show that the metal abundances of the red
stars and the ISM can be easily reconciled.
The plan of the paper is as follows. In Sect. 2 we
present the data reduction and calibration. Section 3
presents color-magnitude diagram in different colors, using
a statistical correction of the foreground contamination.
The CMD location of C stars is also discussed. In Sect. 4
we rederive the distance and metallicity of SagDIG by
assuming a different reddening for the young and old populations. The properties and different spatial distributions
of the blue and red stellar populations are quantified and
discussed in Sect. 5, where the surface density of young
stars in different age intervals is compared with the projected distribution of neutral hydrogen. As a result of the
revised metallicity, SagDIG is shown to fit well the known
luminosity-abundance trend of dwarf irregular galaxies.
Our results are summarized in Sect. 6.
2. Observations and data reduction
Observations of the Sagittarius dwarf irregular were obtained in two runs. SagDIG was first observed on the
photometric night of Sep. 8, 1996, using efosc2 at the
Table 1. The journal of observations.
Night
Sep.
Sep.
Sep.
Sep.
Sep.
Sep.
8, 1996
8, 1996
8, 1996
30, 1999
30, 1999
30, 1999
Tel.
Filter
2.2 m
2.2 m
2.2 m
NTT
NTT
NTT
B
V
I
B
V
I
texp [s]
X
FWHM
×
×
×
×
×
×
1.02
1.05
1.03
1.08
1.08
1.16
1.00 3
1.00 5
1.00 4
1.00 0
1.00 0
0.00 9
2
2
2
4
12
8
900
600
900
300
300
300
ESO/MPI 2.2 m telescope. The efosc2 camera was
equipped with a 2048 × 2048 Loral CCD, with pixel size
of 0.00 26. A readout window was employed to discard the
vignetted edges of the CCD, yielding a useful area of
6.0 9 × 6.0 9. Since the tidal radius of SagDig is only ∼1.0 7
(Mateo 1998), no observations of a separate control field
were needed. A detailed account of the observations and
reduction for this run can be found in our study of the
Phoenix dSph/dI galaxy (Held et al. 1999). The galaxy
was re-observed in better seeing conditions on the night
of 30 Sep. 1999 with the EMMI multi-mode instrument
on the ESO NTT telescope. The sky was marginally photometric with occasionally some thin cirrus. The total exposure times were 1h in V , 20m in B, and 40m in I. The
V and I data were obtained using a 2048×2048 Tektronix
CCD at the red arm of EMMI, with pixel size of 0.24 µm
(0.00 27) and a field of view of 9.0 2 × 9.0 2. The B images
were taken at the blue arm of EMMI, with a 1024 × 1024
Tektronix CCD with a projected pixel size of 0.00 37 and a
smaller field-of-view, 6.0 2 × 6.02. The observing log for both
runs is given in Table 1.
The processing of the images was carried out within
both the iraf and midas environments. After bias subtraction and flat-fielding (using twilight sky flats) all images were registered, and sum images were produced for
each telescope by co-adding all images taken with the same
filter. The programs daophot ii /allstar (Stetson 1987)
were run on the sum images to obtain stellar photometry by point spread function (PSF) fitting. For the NTT
data, we also used the allframe program (Stetson 1994),
which combines PSF photometry carried out on the individual images. The 2.2 m data set was mainly employed
for calibration.
Calibration of the 2.2 m data was based on observations of standard star fields from Landolt (1992). The calibration procedure and color transformations are identical
to those described in Held et al. (1999). The total zero
point errors, including the uncertainties in the calibrations, are 0.012, 0.013, and 0.013 mag in B, V , and I,
respectively.
The NTT data were independently calibrated using
the relations:
B = b0 − 0.126 (B − V ) + 24.890
V = v 0 + 0.017 (B − V ) + 25.113
V = v 0 + 0.017 (V − I) + 25.113
I = i0 − 0.021 (V − I) + 24.411
(1)
(2)
(3)
(4)
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
395
Table 2. The photometric errors (1σ) and completeness from
the artificial star experiments.
BV I
σB
σV
σI
CB
CV
CI
18.8
19.3
19.8
20.3
20.8
21.3
21.8
22.3
22.8
23.3
23.8
24.3
24.8
25.3
0.01
0.01
0.01
0.01
0.01
0.02
0.02
0.03
0.04
0.06
0.08
0.10
0.12
0.18
0.01
0.01
0.01
0.02
0.02
0.03
0.04
0.05
0.07
0.10
0.12
0.13
0.17
0.21
0.01
0.01
0.02
0.02
0.03
0.05
0.06
0.08
0.12
0.15
0.17
0.19
0.23
0.26
0.998
0.999
0.997
0.997
0.992
0.992
0.994
0.985
0.984
0.967
0.956
0.940
0.760
0.550
0.998
0.997
0.997
0.995
0.994
0.989
0.984
0.975
0.963
0.920
0.860
0.670
0.450
0.255
0.994
0.994
0.990
0.990
0.985
0.980
0.970
0.945
0.880
0.825
0.669
0.450
0.278
0.196
where the b0 , v 0 , and i0 magnitudes are the instrumental magnitudes for the standard stars, measured in apertures with radius 6.00 9, normalized to zero airmass and 1 s
exposure. The instrumental PSF magnitudes of stars in
the SagDIG field were converted to normalized aperture
magnitudes using a growth curve analysis of bright isolated stars in the individual images (see Saviane et al.
1996). A comparison of stars in common with the 2.2 m
data set gives the following median zero point differences:
∆B (2.2 m–NTT) = −0.02, ∆V = 0.01, and ∆I = −0.05.
The magnitude scales are therefore in good agreement, especially for the B and V bands. Since the 2.2 m data have
well established calibration zero points, the latter were
adopted as the reference photometric scale. Small adjustments were applied to the NTT data accordingly.
Photometric errors and the completeness were estimated from artificial star experiments. Simulated stars
were added to the sum images by randomly distributing
them around the nodes of a grid of triangles – a procedure
well suited to prevent self-crowding (see Saviane et al.
2000). The frames were then reduced and calibrated as
done for the original images. A comparison of the input
and measured magnitudes for the retrieved stars gives the
internal errors (rms in 0.5 mag bins) and completeness,
which are given in Table 2.
Calibrated magnitudes for the stars in the SagDIG
field were compared with previous photometry to check
the reliability of the zero points. Our results agree with
previous data of C87. The median differences are ∆V =
Vus − VC87 = 0.020 ± 0.024, and ∆(V − I) = 0.030 ± 0.023
(the errors being standard deviations of the residuals).
A direct comparison is not possible with the data of
KAM99, since photometric catalogs have not been published. However, the magnitudes and colors of key features in their CMDs (such as the RGB tip or the blue
plume) are in excellent agreement with those measured in
our diagrams. The (V − I) colors measured by LK00 and
by us show significant disagreement, the median shift be-
B-I
Fig. 1. The V , (B − I) color-magnitude diagram of a field centered on SagDIG (lower panel), compared with the CMD in
the control region (upper panel). Both the inner and outer region have an area 5.0 5×2.0 7. Blue and red stars belonging to the
galaxy, in excess over the foreground contamination, are clearly
visible in the diagram of the inner region. The rectangles delimit two samples of young stars in two different age intervals,
while the slanted box outlines a high-probability sample of red
giant stars.
ing ∆(V − I) = 0.220 ± 0.086 (this paper − LK00). The
blue shift in the (V − I) scale of LK00 significantly affects
their metallicity estimate. A systematic difference is also
present in (B − V ) colors, ∆(B − V ) = 0.100 ± 0.065 (us –
LK00). The V magnitude scales are more nearly consistent, yielding ∆V = −0.040 ± 0.069.
3. The color-magnitude diagrams
The color-magnitude diagram of the inner part of our image, comprising most of the Sagittarius dIrr galaxy, is
shown in Fig. 1 (lower panel). The inner region was defined
as a 5.0 5×2.07 rectangle around SagDIG, with the long side
in the EW direction, and contains both SagDIG’s and foreground stars. The CMD of an outer region of equal area
(upper panel) illustrates the considerable foreground contribution of stars in the Galactic bulge in the direction of
396
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
Fig. 2. The I, (V − I) color-magnitude diagram of SagDIG
after applying statistical decontamination. We have superimposed the C star candidates found by Cook (1987; open
squares) and those identified by Demers & Battinelli (2001;
open triangles).
SagDIG. Despite the field contamination, the blue plume
of young stars and the red giant branch of SagDIG are
evident in the diagram of the inner area. Three CMD regions used to select samples of stars of different ages are
outlined in Fig. 1 – these will be utilized in Sect. 5 to
study the stellar population gradients in the galaxy.
A statistical foreground subtraction procedure was applied to the analysis of the CMDs of SagDIG. All stars in
the CMD of the inner region having a counterpart in the
diagram of the outer field were statistically identified as
interlopers and culled out. The coincidence was tested in
CMD cells 0.3 × 0.3 mag in color and magnitude, respectively. An example of the cleaned CMD of SagDIG is
shown in Fig. 2 (see also Fig. 4).
All evolutionary features are more clearly seen in the
decontaminated diagrams than in the raw CMDs. The
blue plume of young stars is well delineated for more than
4 mag, and the red giant branch shows a well-defined cutoff and extends over a ∼3 mag interval in both V and I.
Several stars populate the Hertzsprung gap. Although
many are likely to be He-burning stars in SagDIG, a fraction of them are possible artifacts caused by the significant
crowding in ground-based data.
Two features are noted in all of our statistically decontaminated diagrams, so that they are likely to be real.
The first is a group of probable red supergiants located
∼2 mag above the RGB tip (Fig. 2). The second feature
is a tail of very red stars with V ∼ 22, V −I >
∼ 1.5, strongly
resembling the extended tail of intermediate-age asymptotic giant branch (AGB) stars found in many dwarf
galaxies. This feature suggests the presence of a significant intermediate-age population.
This conclusion is supported by the remarkable coincidence in magnitude and color with the candidate C stars
found by Cook (1987) and more recently by Demers &
Battinelli (2001) (see Fig. 2). The C star candidates were
classified by Cook (1987) in two groups: a luminous 1 Gyr
old population (reaching ∼2 mag in I above the RGB
tip) and a bluer, less luminous population about 10 Gyr
old. The comparison between old and new measurements
reveals an intrinsic variability of these stars. The crossidentification of C stars is firm, being based on positional coincidence within ±1 pixel (0.00 3). The differences
between Cook’s measurements and ours for candidate C
stars is, after applying a 2σ clipping, ∆V (this paperCook) = 0.23 mag with a standard deviation 0.21 mag.
This scatter is significantly larger than instrumental errors
determined from artificial star experiments (see Table 2).
Also, it is larger than the standard error of the residuals for the general sample of stars in the same CMD region, for which we measured a mean difference 0.02 mag
(us−Cook), with a standard deviation σV = 0.09.
4. Basic properties of SagDIG
In view of the direct dependence of the inferred galaxy
distance and metallicity on the adopted EB−V , before discussing the basic properties of SagDIG we must consider
in some detail the reddening of this galaxy.
4.1. Foreground and internal extinction
Cook (1987) estimated a relatively low reddening in the
direction of SagDIG (EB−V = 0.07) from the color distribution of the Galactic foreground stars. This result agrees
with the prediction from the Hi maps of Burstein & Heiles
(1984), EB−V = 0.08 ± 0.03. The infrared dust emission
maps of Schlegel et al. (1998) suggest a slightly higher
reddening (EB−V = 0.12 ± 0.01). Lee & Kim (2000) used
their (B−V ), (V −I) two-color diagram to infer a very low
reddening for the red giant stars in SagDIG. Reddening
values estimated using these colors, however, are poorly
constrained because the reddening vector is nearly parallel to the stellar sequence. Following Cook (1987), we have
evaluated the extinction in the direction of SagDIG by
comparing the (V −I) color distribution of the foreground
Galactic stars in our database, brighter than V = 22 and
redder than B − I = 0.5, with the colors of stars in the
South Polar Cap (Caldwell & Schecter 1996). The best fit
of the two color distributions (particularly of the blue cutoff at V − I ∼ 0.65 related to the main sequence turnoff
of Galactic disk stars) was obtained by assuming a foreground reddening E(B−V ) = 0.07, with an uncertainty of
about ±0.02 mag. A similar value, E(B − V ) ≈ 0.05, was
obtained by Demers & Battinelli (2001) from the (R − I)
distribution of foreground stars.
Evidence for a higher reddening has been found in
the star forming regions. In their spectroscopic study of
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
397
Hii regions in SagDIG, Skillman et al. (1989b) obtained
c(Hβ) = 0.33. This value was converted into EB−V = 0.22
using the relation c(Hβ) = 1.47 × EB−V (Seaton 1979).
Recent measurements of the Balmer decrement in the
largest Hii region by Saviane et al. (2001) confirms this
high reddening, yielding E(B − V ) = 0.19 ± 0.04. While
this result strictly pertains to the warm ISM, it is likely to
apply also to the young stars in the blue plume, physically
associated to the interstellar gas.
The presence of a differential extinction between young
and old stars is well known in starburst galaxies (e.g.,
Calzetti et al. 1994). Recently formed stars are embedded
in regions of high dust content, while old stars are distributed in more extended morphological structures (halos or disks) (e.g., Zijlstra & Minniti 1999). A differential
reddening has been suggested in some other dIrrs, for instance IC 10 (Sakai et al. 1999). This might well be the
case also for SagDIG, where the young stars are concentrated near the Hi density peaks (see Sect. 5.2), while the
older stars show an extended distribution.
4.2. Distance and metallicity
The I-band magnitude distribution (hereafter LF) of the
red giant stars in SagDIG was obtained from a statistically decontaminated sample of stars selected outside a
radius r = 0.0 9 from the galaxy center. This choice excluded most star-forming regions, yielding a clean subsample of red giants in the “halo” of SagDIG (Fig. 3).
The LF was derived by simply counting stars in the color
range 0.8 < V − I < 1.8.
The clear RGB cutoff seen in the LF was identified as
the tip of the red giant branch, and employed to derive the
distance to SagDIG according to the iterative methods of
Mould & Kristian (1986) and Lee et al. (1993) (see Held
et al. 1999). The RGB tip location was measured by filtering the luminosity function with a Sobel kernel (see, e.g.,
Madore & Freedman 1998 and references therein). This
method yielded Itip = 21.30 ± 0.15, where the uncertainty
includes the internal error (assumed to be half the bin size)
and the calibration errors. As a check, we also measured
the RGB cutoff by fitting an error-convolved step function
to the magnitude distribution, obtaining the same result.
Our estimate of the tip level is therefore slightly brighter
than that obtained by KAM99 (Itip = 21.38), although
the difference is within the quoted errors.
The initial guess of the distance was based on the assumption that MIRGBT = −4.0, which is an excellent approximation for metal-poor systems, where the I luminosity of the RGB tip shows only a modest dependence
on the galaxy metallicity (see also Salaris & Cassisi 1998;
Bellazzini et al. 2001). Our distance estimate assumes a
low reddening (EB−V = 0.07 ± 0.05, EV −I = 0.09 ± 0.06,
AI = 0.13 ± 0.10) for the RGB population, and a mean
metallicity [Fe/H] = −2.08 ± 0.20 dex (see below). With
these assumptions, we obtained a corrected distance modulus (m − M )0 = 25.14 ± 0.18 (1.07 ± 0.09 Mpc), a value
Fig. 3. The I, (V − I) color-magnitude diagram of a sample
of SagDIG stars with distance from the galaxy center r > 0.0 9.
The red giant stars in SagDIG are nearly as metal-poor as those
in the Galactic globular cluster M 15 ([Fe/H] = −2.17, solid
line), and more metal-poor than stars in M 2 ([Fe/H] = −1.58,
dashed line). We use a distance modulus (m − M ) = 25.14 and
a reddening EB−V = 0.07 for SagDIG.
confirming previous estimates. The distance error includes
all uncertainties on the RGB tip magnitude, reddening
and metallicity through standard error propagation.
The mean [Fe/H] of the “old” stellar population in
SagDIG was estimated as in Saviane et al. (1996), by comparing the colors of the red giants with the RGB fiducial
sequences of template Galactic globular clusters (GGC).
The adopted reddening values are those specified above.
The average color differences between the RGB stars in
SagDIG and the GGC fiducials, measured in the interval
21.3 < I < 22.3, were measured using the cluster ridge
lines and metallicities of Da Costa & Armandroff (1990).
A quadratic fit to the relation between mean color shifts
and GGC metallicities yields [Fe/H] = −2.08 for SagDIG.
The uncertainty, computed from the error on the color
difference, is about 0.20 dex.
The metallicity obtained for SagDIG is among the lowest for dwarf galaxies, yet less extreme than found by previous authors. Had we adopted a reddening EB−V = 0.12
(i.e. EV −I = 0.15) as in KAM99, a mean [Fe/H] = −2.31
would have been obtained, which indicates that our metalliciy estimate and that of KAM99 are essentially consistent given the different assumption for the reddening. The
much lower metallicity range inferred by LK00 is most
likely related to the photometric zero points adopted by
these authors, yielding (V − I) colors which are systematically bluer than those obtained by C87, KAM99, and
this study.
398
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
Table 3. Properties of stars projected onto the Hii regions.
region
shk
shk
shk
shk
shk
Fig. 4. The color-magnitude diagram of young stars in
SagDIG, with superposed model isochrones with Z = 0.0004
and ages ∼10, 30, and 100 Myr (from Bertelli et al. 1994).
We adopt a reddening EB−V = 0.19, appropriate for the starforming regions, and an apparent distance modulus 25.73. The
thin lines represent the core H burning phase, while the thick
lines represent the faster post-MS stages. Large filled circles
represent three stars identified in the largest Hii region, while
the two starred symbols are objects coincident with the two
smaller Hii region candidates.
5. Stellar populations
5.1. The recent star formation
Figure 4 shows a statistically cleaned color-magnitude diagram with superimposed a set of theoretical isochrones
with ages 10, 30, and 100 Myr. The isochrones are
Z = 0.0004 models ([Fe/H] = −1.7) from Bertelli et al.
(1994). A thick line emphasizes the He burning part
of the isochrones. The CMD was transformed into the
MV , (B − I)0 plane by adopting a true distance modulus 25.14 (see previous section) and a reddening appropriate for the star forming regions (EB−V = 0.19 ± 0.05,
AV = 0.59 ± 0.10). The apparent distance modulus is
therefore 25.73 mag.
The general picture of star formation is quite similar
to that delineated by previous work. However, the cleaner
CMD allowed by our statistical decontamination, together
with the larger photometric baseline, provide new interesting pieces of information on the SFH of SagDIG. First,
the blue-loops of the 30 Myr isochrone match quite well
the luminosity and color of the two groups of blue and red
stars near MV ' −5.5. This supports the reality of the red
group and its identification as a clump of red supergiants.
According to the Padua models, such age implies a MS
turnoff mass ∼9 M . Secondly, the blue stars in the range
−5 < MV < −4 appear perhaps too blue for He burning
1
2
3
3
3
star
x
y
V
B−V
V −I
12850
14120
12880
12820
13150
875.9
859.9
1182
1166
1185
790.0
869.8
792.5
788.1
809.6
18.01
19.28
21.35
22.21
21.92
0.77
0.14
−0.18
0.05
−0.16
0.89
0.47
−0.19
0.49
−0.10
stars, as KAM99 suggested – it is quite possible that they
are MS stars slightly older than 10 million year. Further,
we note the absence of a prominent plume of red supergiants that should be expected to define the red side of
the blue loops. HST observations may eventually clarify
this issue. Also, the obvious shortage of stars with age between 30 and 100 Myr suggests that the star formation
rate dropped nearly 100 million years ago, with a short
burst of star formation about 30 Myr ago interrupting a
relatively quiescent period.
Finally, we remark the presence of a few very bright
stars spatially coincident with the candidate Hii regions
investigated by Strobel et al. (1991) (Table 3). Two bright
objects (MV < −6) were found in each of the two smaller
candidate Hii regions (#1 and #2). These objects have
been classified as probably galactic, given the absence of
[Oiii] emission (Skillman et al. 1989b). The brightest one
(in region SHK 1) is quite red, which is consistent with
the identification with a foreground dwarf star. The color
of the star coincident with region SHK 2 is consistent with
a supergiant or a star clusters unresolved in ground-based
data (see Cappellari et al. 1999). Three stars coincident
in space with the bona-fide Hii region (#3) are luminous
and hot enough to represent possible exciting stars. They
are as luminous as expected for ∼20 Myr main-sequence
stars (MV ∼ −4, large circles in Fig. 4).
5.2. Spatial distributions: young stars vs. red giants
Stars of different ages in SagDIG are distributed in a very
different way across the galaxy. Previous studies, starting
with Cook (1987), had already noted that blue stars are
only found in the central regions of SagDIG. In the following, we will show that the youngest stars are embedded in
a region of high Hi density, while the older populations are
located away from the galaxy center, forming an extended
halo or disk with a radial exponential fall-off.
Figure 5 shows the spatial distribution of stars in different age intervals, superimposed onto the surface density
distribution of the neutral gas (from Young & Lo 1997).
The latter authors showed that the ISM of SagDIG comprises a broad, warm component (σ = 10 km s−1 ) and a
narrow, cold one (σ = 5 km s−1 ), with the warm component distributed throughout the galaxy (out to 3 Kpc from
the center) while the cold one is concentrated into a small
number of clumps of ∼8 × 105 M . A prominent clump
is nearly coincident with the biggest Hii region (Strobel
et al. 1991).
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
399
Fig. 5. The spatial distribution of young and old stars in SagDIG superimposed on the surface density map of Hi from Young
& Lo (1997). a) The most luminous blue stars in SagDIG, including both MS and BL stars; b) main sequence stars with age
between 40 and 200 Myr; c) the carbon stars candidates from Cook (1987, crosses) and Demers & Battinelli (2001, squares);
d) red giant branch stars as selected in Fig. 1. The field size of each panel is 8.5 arcmin. N is to the top, E to the left.
The color and magnitude selections are those outlined
in Fig. 1; no further statistical decontamination or spatial
selection was applied. Two boxes sharing the color interval
−0.5 < B−I < 0.5 were used to pick up MS stars approximately between 20–80 Myr (21.8 < V < 24.0) and younger
than 20 Myr (19.4 < V < 21.8), respectively. Both regions
will also contain a fraction of He burning stars on the blue
loops, somewhat older than MS stars at a given luminosity. For example, the blue stars in the brighter subsample
are a mixture of MS stars younger than 20 Myr and He
burning stars with age <100 Myr.
The distributions of the young stars in both age intervals are plotted in Figs. 5a and b. The location of the
youngest stars (panel a) indicates that the most recent
star formation episode occurred in a small region located
between the two brightest Hi clumps along the gaseous
shell, somewhat offset from the Hi hole. The size of this
association is ∼0.0 5 (180 pc).
The less young stars show a clumpy distribution
around the same region, with a lower central concentration and a spatial extent of the order 20 in diameter
(∼600 pc). If we make the hypothesis that the young stars
retain the velocity dispersion of the cold, dense Hi clumps
from which they probably originated, this size appears
consistent with star diffusion in >
∼100 Myr. Indeed, with
a stellar velocity dispersion of about 5 km s−1 , equal to
that of the narrow Hi component (Young & Lo 1997),
the crossing time of a 0.5 Kpc region is 100 Myr. Note,
however, that the asymmetric shape of the star forming
region in Fig. 5b, as well as the presence of several clumps
in the distribution of young stars, suggest the occurrence
of stochastic star formation associated with the Hi shell.
Probably what we are seeing is the result of a combination of the two mechanisms. We finally note that some
blue stars are found in “tails”, perhaps a hint of spiral
structure, quite far from the main star-forming site. This
may be the signature of star formation on the rim of the
shell.
In contrast to the distribution of the young stars, the
red giants in SagDIG are uniformly distributed across the
galaxy (Fig. 5d), with their mean position approximately
coincident with that of the blue stars. Interestingly, we
note a degree of coincidence with the ridges and arms in
the distribution of neutral gas, which appears more than
fortuitous – e.g., note the arm-like filaments of stars tracing the western rim of the Hi shell. These red stars need
not be very old: they may well be relatively young red giants (yet older then 1 Gyr), as it is probably the case in
400
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
5.3. The metallicity-luminosity relation
Fig. 6. The surface density profiles of young stars (open
squares) and red giant stars (filled circles) in SagDIG. The
straight lines represent exponential fits to the density distribution of young and old stars. Note the larger scale length of the
extended halo of red stars surrounding the inner, star-forming
regions of SagDIG.
Leo A (Tolstoy et al. 1998). The intermediate-age upperAGB population seems to share the extended distribution
of the red giants, as it can be seen from the distribution
of C stars in the samples of Cook (1987) and Demers &
Battinelli (2001) (Fig. 5c).
Figure 6 shows the different surface density profiles of
blue stars (younger than about 80 Myr; 19.4 < V < 24.0)
and red giants. The profiles are plotted against the distance from the galaxy center, defined as the mean x, y
of red giants. Both profiles are nearly exponential as expected in dwarf galaxies. It is apparent from this figure
that the radial scale length of the RGB stars is larger
than for the blue stars. A linear fit in the radial range
1.0 2 < r < 3.0 8 (0.4–1.2 Kpc) provides a quantitative estimation of the different exponential scale lengths of young
and “old” stars. The scale lengths are 4600 and 3300 (0.24
and 0.17 Kpc) for the red giants and blue stars, respectively. The global scale lengths measured by KAM99 and
LK00 are clearly dominated by the young stars. The central flattening of the RGB star profile is quite uncertain in
the innermost 0.3 Kpc, because of incompleteness in the
star counts caused by the extreme crowding. In particular,
the red stars are likely to be masked by the more luminous
young star complexes. Overall, there are several hints that
SagDIG may be a disk galaxy seen nearly face-on, owing
its irregular shape to the optical signatures of recent star
formation. The rotation required to support such a lowmass galaxy is very small, and could easily be masked by
the turbulent gas motions (see Young & Lo 1997).
The metallicity estimated in Sect. 4.2 for the red giant
stars in SagDIG ([Fe/H] ' −2.1) turns out to be in good
agreement with the metal content estimated for the ISM.
A new determination of the oxygen abundance in the
Hii regions of SagDIG is presented in a companion paper
(Saviane et al. 2001). The new estimate, 12 + log(O/H) =
7.23 ± 0.20, revises downwards the [O/H] determination of
Skillman et al. (1989b), yielding (under the same physical
assumptions) a value more metal-poor by about 0.2 dex.
We have transformed this result to [Fe/H] = −2.07 ± 0.20
by adopting 12 + log(O/H) = 8.93 for the solar O abundance, and using the mean difference between [Fe/H] and
[O/H] given by Mateo (1998). Under these assumptions,
the composition of the warm gas in the Hii regions does
not appear to be significantly metal enriched with respect
to the red giant stars.
These new estimates of the mean metallicity of both
the red giant star population and the warm ISM in
SagDIG are compared with the properties of other dwarfs
in the metallicity–luminosity diagram. Figure 7 shows
a plot of both stellar [Fe/H] and nebular [O/H] measurements (see Skillman et al. 1989a) against luminosity
for a large sample of dwarf galaxies. The SagDIG data
point was plotted using our estimates of mean metallicity and the MV measured by KAM99. The data are
mostly from Mateo (1998) and van den Bergh (2000).
SagDIG now appears to be consistent with the general
trend of metallicity against luminosity for dwarf irregulars. Its metallicity, although less extreme than found by
previous studies, remains the lowest among Local Group
galaxies, and shares the tendency of low-luminosity dIrrs
(e.g., UKS 2323-326: Lee & Byun 1999; WLM: Minniti
& Zijlstra 1997; Sextans A: van Dyk et al. 1998) to a
lower stellar metallicity than dSph galaxies of comparable luminosities. Whether this trend is really produced by
a bimodal metallicity, or rather is due to the fact that
RGB stars may have a younger age in dIrrs than in dwarf
spheroidals, is still matter of debate.
6. Summary and conclusions
We have presented a BV I study of the stellar content
and metallicity of UKS 1927-177, the Sagittarius dwarf
irregular galaxy, based on deep color-magnitude diagrams.
We have found that the color-magnitude diagram of
SagDIG is better understood by introducing a differential
reddening scenario in which the young stars, located near
high-density Hi clumps, are more reddened than the older
stars distributed all over the galaxy. In fact, the color distribution of the Galactic foreground stars indicates a relatively low reddening (we assume EB−V = 0.07 ± 0.02 for
the old stars), while measurements of the Balmer decrement in Hii regions (Skillman et al. 1989b; Saviane et al.
2001) provide a higher reddening, EB−V = 0.19. Using the
lower reddening for the “old” population in SagDIG, we
obtained revised values for the metallicity and distance,
Y. Momany et al.: The SagDIG dwarf: Metallicity and stellar populations
401
a group of candidate red supergiants that are quite well
fitted by the isochrones of young He-burning stars.
We have also obtained a detailed quantitative comparison of the spatial distribution of stars in different age
ranges with the distribution of the ISM. Different density
profile scale lengths have been measured for the young
blue stars and the red giants. The youngest stars have
been shown to concentrate in a central region nearly coincident with the density peaks in the Hi distribution. In
constrast, the distribution of red giants is quite extended,
yet it seems to be correlated with the HI morphology as
well. This may suggest for the red giants in SagDIG a contribution by relatively young (a few Gyr old) stars. We also
noted that some blue stars are found in “tails”, perhaps
a hint of spiral structures, quite far from the main starforming sites. This suggests a similarity with the small
spiral-like structures that can form even in a small galaxy
according to the theory of stochastic self-propagating star
formation (Gerola & Seiden 1978). An alternative possibility is that these features are a vestige of star formation
related to the gaseous shell.
Fig. 7. Metallicities of stars and the ISM of dwarf galaxies in
the Local Group and beyond, plotted against their V absolute
magnitude. References to data are given in the text. Upper
panel: crosses refer to dSph galaxies, open squares are the dE
companions to M 31, the filled square is the data point for the
low-luminosity elliptical M 32, filled circles are dwarf irregulars, and triangles represent “transition” galaxies (dSph/dI)
(see Mateo 1998). SagDIG is represented by the data point with
error bars. Lower panel: the [O/H] abundances of the gaseous
component, measured from nebular emission lines. The symbols are the same as for the stellar metallicities. Stars represent dwarf irregulars or blue compact dwarfs outside the Local
Group.
[Fe/H] = −2.1 ± 0.2 and (m − M )0 = 25.14 ± 0.18, respectively. While the distance confirms previous estimates,
our metallicity turns out to be significantly higher than
those proposed by Karachentsev et al. (1999) and Lee
& Kim (2000). Using this new metallicity, we have compared SagDIG with other dwarf galaxies in the luminositymetallicity diagram, and found that it is consistent with
the general trend for dIrr galaxies.
The large baseline given by the (B − I) color, together
with an analysis based on statistical subtraction of the
Galactic foreground, provided additional information on
the recent star formation in SagDIG. The C stars from two
sources have also been compared with our cleaned CMDs,
which confirmed the presence of an intermediate age population. For the young stellar population, we have adopted
the reddening derived for the Hii regions, thus obtaining
a good match to the theoretical isochrones. A comparison with models indicates a significant burst taking place
∼30 Myr ago, with star formation going on until ∼10 Myr
ago. This burst seems to have interrupted a relatively quiescent period between ∼30–100 Myr ago. We identified
Acknowledgements. We thank F. Bresolin for useful comments on an early draft, and the anonymous referee for helpful remarks that improved the presentation of this paper.
This research has made use of the NASA/IPAC Extragalactic
Database (NED) and of NASA’s Astrophysics Data System
Service.
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